热控涂层电子辐照效应

研究防静电Kapton二次表面镜(ITO/Kapton/Al)、S781白漆两种典型热控涂层,在不同能量电子辐照后太阳吸收比退化情况,并利用X射线光电子能谱和扫描电子显微镜对样品表面的成分和形貌进行了分析。结果表明:相同电子注量下,不同能量电子对样品的太阳吸收比退化作用程度是有区别的。而样品光谱反射率、表面形貌、表面成分的损伤效应类似,说明不同能量电子辐照下,样品的退化机理是一致的。     

民航行李X光安检图像自适应小波去噪算法

对X光安检图像进行去噪处理可以更清楚地显示出危险物。针对传统小波软硬阈值去噪方法的缺陷．给出了一种自适应阈值的去噪方法,在此方法中,首先进行软硬阈值的折中处理,然后分别对大于和小于阈值的两部分进行自适应处理。利用Tennessee大学提供的实际采集的X光安栓图像进行实验,结果表明该方法能有效地去除安检图像中的噪声,图像去噪后的信噪比、峰值信噪比分别是25．2229dB、27．708dB．与含噪图像相比分别增加了7．7253dB和7．739dB。因此该方法表现出较高的去噪性能。     

机身前体横截面形状对三角翼涡破裂位置的影响

通过求解三维定常雷诺时均方程,采用剪切应力输运(SST)湍流模型,在亚声速范围内,分别对融合体前体-三角翼组合体和旋成体前体-三角翼组合体流场中翼涡破裂现象进行了数值模拟.模拟结果显示:与旋成体前体相比,在中、大迎角时,融合体前体的分离涡,涡量集中、强度高,进入机翼上方流场后,能够与翼涡密切耦合,彻底地改变翼涡强度的分...     

酚醛树脂固化度的X射线衍射分析

发展使用Ｘ射线衍技术对酚醛树脂固化度进行研究，确定了酚醛树脂固化度与Ｘ射线散射最大值的 关系，得出了利用２θ角来标定树脂固化度的公式。该方法具有快速、无损、灵敏度主同的优点，并可适用于各种不同的酚醛树脂。     

用X光电子能谱研究复合固体推进剂燃烧机理

本文介绍了X光电子能谱(XPS)分析技术在复合固体推进剂燃烧机理研究中的应用。用XPS分析对一种呈负压力指数燃烧特性的聚氨酯复合固体推进剂(404-5A)的未然表面和在2、2.5、3.0、3.5、4.0MPa压强下快速降压熄火后的燃烧表面作元素组成及其化学价态的分析,得到了不同价态的各元素原子百分含量。从实验结果可以确定CaCO_3在凝相反应中生成了CaCl_2。从燃面上碳原子浓度随燃烧压强的变化说明了燃烧过程中存在着熔化的粘合剂对过氯酸铵表面的流动覆盖,覆盖程度随着燃烧压强的上升而增加。本文还对CaCO_3、粘合剂流动覆盖在燃烧过程中的作用进行了探讨。     

Broadening of Fe X (6374 Å) profiles above the limb in a coronal hole

Profiles of the visible Fe X (6374 Å) coronal emission line as a function of height above the limb were obtained out to 1.16 solar radii in a coronal hole using the NSO/Sacramento Peak Observatory Coronagraph, Universal Spectrograph and a CCD camera. These are the first coronal line profiles obtained as a function of height in a coronal hole from the ground. Analysis of the line widths suggests a large component of nonthermal broadening which increases with height ranging from 40 to 60 km/s, depending upon the assumed temperature or thermal component of the profile.     

带有太阳电池阵的卫星电源系统在轨测试方法

根据带有太阳帆板的地球同步卫星在轨测试需求,分析了星上电源系统的组成及技术状态;并以光照区可调节母线为例。给出了卫星电源系统在轨测试方法及相应的计算公式;最后,通过工程验证了该方法的正确性。     

A Comparative Study of the Influence of the Active Young Sun on the Early Atmospheres of Earth, Venus, and Mars

Because the solar radiation and particle environment plays a major role in all atmospheric processes such as ionization, dissociation, heating of the upper atmospheres, and thermal and non-thermal atmospheric loss processes, the long-time evolution of planetary atmospheres and their water inventories can only be understood within the context of the evolving Sun. We compare the effect of solar induced X-ray and EUV (XUV) heating on the upper atmospheres of Earth, Venus and Mars since the time when the Sun arrived at the Zero-Age-Main-Sequence (ZAMS) about 4.6 Gyr ago. We apply a diffusive-gravitational equilibrium and thermal balance model for studying heating of the early thermospheres by photodissociation and ionization processes, due to exothermic chemical reactions and cooling by IR-radiating molecules like CO₂, NO, OH, etc. Our model simulations result in extended thermospheres for early Earth, Venus and Mars. The exospheric temperatures obtained for all the three planets during this time period lead to diffusion-limited hydrodynamic escape of atomic hydrogen and high Jeans’ escape rates for heavier species like H₂, He, C, N, O, etc. The duration of this blow-off phase for atomic hydrogen depends essentially on the mixing ratios of CO₂, N₂ and H₂O in the atmospheres and could last from ∼100 to several hundred million years. Furthermore, we study the efficiency of various non-thermal atmospheric loss processes on Venus and Mars and investigate the possible protecting effect of the early martian magnetosphere against solar wind induced ion pick up erosion. We find that the early martian magnetic field could decrease the ion-related non-thermal escape rates by a great amount. It is possible that non-magnetized early Mars could have lost its whole atmosphere due to the combined effect of its extended upper atmosphere and a dense solar wind plasma flow of the young Sun during about 200 Myr after the Sun arrived at the ZAMS. Depending on the solar wind parameters, our model simulations for early Venus show that ion pick up by strong solar wind from a non-magnetized planet could erode up to an equivalent amount of ∼250 bar of O⁺ ions during the first several hundred million years. This accumulated loss corresponds to an equivalent mass of ∼1 terrestrial ocean (TO (1 TO ∼1.39×10²⁴ g or expressed as partial pressure, about 265 bar, which corresponds to ∼2900 m average depth)). Finally, we discuss and compare our findings with the results of preceding studies.     

The Genesis Solar Wind Concentrator Target: Mass Fractionation Characterised by Neon Isotopes

The concentrator on Genesis provided samples of increased fluences of solar wind ions for precise determination of the oxygen isotopic composition. The concentration process caused mass fractionation as a function of the radial target position. This fractionation was measured using Ne released by UV laser ablation and compared with modelled Ne data, obtained from ion-trajectory simulations. Measured data show that the concentrator performed as expected and indicate a radially symmetric concentration process. Measured concentration factors are up to ∼30 at the target centre. The total range of isotopic fractionation along the target radius is 3.8%/amu, with monotonically decreasing ²⁰Ne/²²Ne towards the centre, which differs from model predictions. We discuss potential reasons and propose future attempts to overcome these disagreements.     

7085铝合金残余应力及加工变形的数值仿真与试验

毛坯残余应力的测量以及零件的加工变形分析是航空整体结构件数控加工工艺研究的难题。应用MSC.Marc软件对某型飞机主起支撑接头的7085铝合金锻件毛坯的淬火-压缩工艺进行了数值仿真,获得了毛坯残余应力分布趋势;应用X射线衍射法与钻孔法测量了毛坯表层残余应力分布,提出了基于系数修正法的毛坯残余应力分析方法,通过最小二乘法（LSM）拟合仿真值与试验值以获得应力修正系数,并对毛坯残余应力分布的仿真结果进行修正,获得了实际毛坯的残余应力分布;由此进行了主起支撑接头缩比零件加工变形仿真与验证试验。研究结果表明：7085铝合金块状毛坯残余应力数值仿真结果与测试结果的趋势吻合,为应力修正提供了物理基础;相对于未修正的应力分布,基于修正后的应力分布仿真获得的变形结果精度提高了50%;7085-T7452铝合金的毛坯残余应力是导致主起支撑接头加工变形的主要因素。